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1. First results from the JWST Early Release Science Program Q3D: Ionization cone, clumpy star formation and shocks in a $z=3$ extremely red quasar host

Author

Vayner, Andrey, Zakamska, Nadia L., Ishikawa, Yuzo, Sankar, Swetha, Wylezalek, Dominika, Rupke, David S. N., Veilleux, Sylvain, Bertemes, Caroline, Barrera-Ballesteros, Jorge K., Chen, Hsiao-Wen, Diachenko, Nadiia, Goulding, Andy D., Greene, Jenny E., Hainline, Kevin N., Hamann, Fred, Heckman, Timothy, Johnson, Sean D., Murphree, Grey, Lim, Hui Xian Grace, Liu, Weizhe, Lutz, Dieter, Lützgendorf, Nora, McCrory, Ryan, Mainieri, Vincenzo, Nesvadba, Nicole P. H., Ogle, Patrick, Sturm, Eckhard, and Whitesell, Lillian

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

Massive galaxies formed most actively at redshifts $z=1-3$ during the period known as `cosmic noon.' Here we present an emission-line study of an extremely red quasar SDSSJ165202.64+172852.3 host galaxy at $z=2.94$, based on observations with the Near Infrared Spectrograph (NIRSpec) integral field unit (IFU) on board JWST. We use standard emission-line diagnostic ratios to map the sources of gas ionization across the host and a swarm of companion galaxies. The quasar dominates the photoionization, but we also discover shock-excited regions orthogonal to the ionization cone and the quasar-driven outflow. These shocks could be merger-induced or -- more likely, given the presence of a powerful galactic-scale quasar outflow -- these are signatures of wide-angle outflows that can reach parts of the galaxy that are not directly illuminated by the quasar. Finally, the kinematically narrow emission associated with the host galaxy presents as a collection of 1 kpc-scale clumps forming stars at a rate of at least 200 $M_{\odot}$ yr$^{-1}$. The ISM within these clumps shows high electron densities, reaching up to 3,000 cm$^{-3}$ with metallicities ranging from half to a third solar with a positive metallicity gradient and V band extinctions up to 3 magnitudes. The star formation conditions are far more extreme in these regions than in local star-forming galaxies but consistent with that of massive galaxies at cosmic noon. JWST observations reveal an archetypical rapidly forming massive galaxy undergoing a merger, a clumpy starburst, an episode of obscured near-Eddington quasar activity, and an extremely powerful quasar outflow simultaneously., Comment: 19 pages, 8 figures. Submitted for publication in ApJ

Published
2023
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2. The GRAVITY+ Project: Towards All-sky, Faint-Science, High-Contrast Near-Infrared Interferometry at the VLTI

Author

Collaboration, GRAVITY+, Abuter, Roberto, Alarcon, Patricio, Allouche, Fatme, Amorim, Antonio, Bailet, Christophe, Bedigan, Helen, Berdeu, Anthony, Berger, Jean-Philippe, Berio, Philippe, Bigioli, Azzurra, Blaho, Richard, Boebion, Olivier, Bolzer, Marie-Lena, Bonnet, Henri, Bourdarot, Guillaume, Bourget, Pierre, Brandner, Wolfgang, Cardenas, Cesar, Conzelmann, Ralf, Comin, Mauro, Clénet, Yann, Courtney-Barrer, Benjamin, Dallilar, Yigit, Davies, Ric, Defrère, Denis, Delboulbé, Alain, Delplancke-Ströbele, Françoise, Dembet, Roderick, de Zeeuw, Tim, Drescher, Antonia, Eckart, Andreas, Édouard, Clemence, Eisenhauer, Frank, Fabricius, Maximilian, Feuchtgruber, Helmut, Finger, Gert, Schreiber, Natascha M. Förster, Fuenteseca, Eloy, Garcia, Enrique, Garcia, Paulo, Gao, Feng, Gendron, Eric, Genzel, Reinhard, Gil, Juan Pablo, Gillessen, Stefan, Gomes, Tiago, Gonté, Frédéric, Gouvret, Carole, Guajardo, Patricia, Guidolin, Ivan, Guieu, Sylvain, Guzmann, Ronald, Hackenberg, Wolfgang, Haddad, Nicolas, Hartl, Michael, Haubois, Xavier, Haußmann, Frank, Heißel, Gernot, Henning, Thomas, Hippler, Stefan, Hönig, Sebastian, Horrobin, Matthew, Hubin, Norbert, Jacqmart, Estelle, Jocou, Laurent, Kaufer, Andreas, Kervella, Pierre, Kirchbauer, Jean-Paul, Kolb, Johan, Korhonen, Heidi, Kreidberg, Laura, Krempl, Peter, Lacour, Sylvestre, Lagarde, Stephane, Lai, Olivier, Lapeyrère, Vincent, Laugier, Romain, Bouquin, Jean-Baptiste Le, Leftley, James, Léna, Pierre, Lewis, Steffan, Lutz, Dieter, Magnard, Yves, Mang, Felix, Marcotto, Aurelie, Maurel, Didier, Mérand, Antoine, Millour, Florentin, More, Nikhil, Nowack, Hugo, Nowak, Matthias, Oberti, Sylvain, Olivares, Francisco, Ott, Thomas, Pallanca, Laurent, Paumard, Thibaut, Perraut, Karine, Perrin, Guy, Petrov, Romain, Pfuhl, Oliver, Pourré, Nicolas, Rabien, Sebastian, Rau, Christian, Riquelme, Miguel, Robbe-Dubois, Sylvie, Rochat, Sylvain, Salman, Muhammad, Scherbarth, Malte, Schöller, Markus, Schubert, Joseph, Schuhler, Nicolas, Shangguan, Jinyi, Shchekaturov, Pavel, Shimizu, Taro, Scheithauer, Silvia, Sevin, Arnaud, Soenke, Christian, Soulez, Ferreol, Spang, Alain, Stadler, Eric, Straubmeier, Christian, Sturm, Eckhard, Sykes, Calvin, Tacconi, Linda, Tischer, Helmut, Tristram, Konrad, Vincent, Frédéric, von Fellenberg, Sebastiano, Uysal, Sinem, Widmann, Felix, Wieprecht, Ekkehard, Wiezorrek, Erich, Woillez, Julien, Yazıcı, Şenol, and Zins, Gérard

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The GRAVITY instrument has been revolutionary for near-infrared interferometry by pushing sensitivity and precision to previously unknown limits. With the upgrade of GRAVITY and the Very Large Telescope Interferometer (VLTI) in GRAVITY+, these limits will be pushed even further, with vastly improved sky coverage, as well as faint-science and high-contrast capabilities. This upgrade includes the implementation of wide-field off-axis fringe-tracking, new adaptive optics systems on all Unit Telescopes, and laser guide stars in an upgraded facility. GRAVITY+ will open up the sky to the measurement of black hole masses across cosmic time in hundreds of active galactic nuclei, use the faint stars in the Galactic centre to probe General Relativity, and enable the characterisation of dozens of young exoplanets to study their formation, bearing the promise of another scientific revolution to come at the VLTI., Comment: Published in the ESO Messenger

Published
2022
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3. The Core of the Matter — Spatially Resolving Active Galactic Nuclei with GRAVITY

Author

GRAVITY Collaboration, Sturm, Eckhard, Cao, Yixian, Clenet, Yann, Davies, Ric, Dexter, Jason, Eckart, Andreas, Eisenhauer, Frank, Genzel, Reinhard, Gratadour, Damien, Hönig, Sebastian, Kishimoto, Makoto, Lacour, Sylvestre, Lutz, Dieter, Millour, Florentin, Netzer, Hagai, Perrin, Guy, Peterson, Brad, Petrucci, Pierre-Olivier, Pfuhl, Oliver, Prieto, M. Almudena, Rouan, Daniel, Santos, Daryl, Shangguan, Jinyi, Shimizu, Taro, Stock, Matthias Raphael, Waisberg, Idel, Woillez, Julien, De Zeeuw, Tim, Amorim, Antonio, Brandner, Wolfgang, Garcia, Paolo J. V., Gillessen, Stefan, Förster Schreiber, Natascha M., Ott, Thomas, Paumard, Thibaut, Perraut, Karine, Straubmeier, Christian, Tacconi, Linda. J., Sternberg, Amiel, and Tristram, Konrad R. W.

Abstract

Thanks to the superb sensitivity and resolution of GRAVITY, ESO’s near-infrared beam combiner for the Very Large Telescope Interferometer, our Large Programme study of the inner regions of active galactic nuclei (AGN) has delivered several recent breakthroughs. We have spatially resolved the broad line region (BLR) for three nearby AGN, supporting the rotating disc model, directly measuring the masses of their supermassive black holes (SMBHs), and testing the BLR radius-luminosity (R-L) scaling relation. We have measured the hot dust sizes for eight AGN and fully imaged the hot dust structure for two AGN. Our dust sizes also test the hot dust R-L scaling relation, revealing the first evidence for luminosity-dependent deviations from the expected relation. The novel GRAVITY data provide unique insight into the physics around SMBHs. In addition, they test the basic assumptions behind mass measurements based on the R-L scaling relation and reverberation mapping, which is currently the only method for measuring black hole masses in large surveys and out to high redshift. Our observations provide an entirely new, independent method for measuring SMBH masses. With GRAVITY+, we will be able to vastly expand to both larger samples and higher redshifts with the ultimate goal of tracing black hole growth and galaxy coevolution through cosmic time., Published in The Messenger vol. 188, pp. 20-25, September 2022.

Published
2022
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4. The Elusive ISM of Dwarf Galaxies: Excess Submillimetre Emission and CO-Dark Molecular Gas

Author

Madden, Suzanne C., Galametz, Maud, Cormier, Diane, Lebouteiller, Vianney, Galliano, Frederic, Hony, Sacha, Remy, Aurelie, Sauvage, Marc, Contursi, Alessandra, Sturm, Eckhard, Poglitsch, Albrecht, Pohlen, Michael, Smith, M. W. L., Bendo, George, O'Halloran, Brian, 2, The SPIRE SAG, consortia., PACS, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Cambridge [UK] (CAM), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, aucun, Macif, Max-Planck-Institut für Extraterrestrische Physik (MPE), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, School of Physics and Astronomy [Cardiff], Cardiff University, University of Manchester [Manchester], Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Metallicity, FOS: Physical sciences, Astrophysics, Photodissociation region, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Low density, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, QB, 0105 earth and related environmental sciences, Line (formation), Dwarf galaxy, Physics, Star formation, General Engineering, Astronomy and Astrophysics, Galaxy, Space observatory, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Herschel Dwarf Galaxy Survey investigates the interplay of star formation activity and the the metal-poor gas and dust of dwarf galaxies using FIR and submillimetre imaging spectroscopic and photometric observations in the 50 to 550mu window of the Herschel Space Observatory. The dust SEDs are well constrained with the new Herschel and MIR Spitzer data. A submillimetre excess is often found in low metallicity galaxies, which,if tracing very cold dust, would highlight large dust masses not easily reconciled in some cases, given the low metallicities and expected gas-to-dust mass ratios. The galaxies are also mapped in the FIR fine-structure lines (63 and 145mu OI, 158mu CII, 122 and 205mu NII, 88mu OIII) probing the low density ionised gas, the HII regions and photodissociation regions. While still early in the Herschel mission we can already see, along with earlier studies, that line ratios in the metal-poor ISM differ remarkably from those in the metal-rich starburst environments. In dwarf galaxies, L[CII]/L(CO) (>10^4) is at least an order of magnitude greater than in the most metal-rich starburst galaxies. The enhanced [CII] arises from the larger photodissociation region where H2, not traced by the CO, can exist. The 88mu [OIII] line usually dominates the FIR line emission over galaxy-wide scales in dwarf galaxies, not the 158mu [CII] line which is the dominant FIR cooling line in metal-rich galaxies. All of the FIR lines together can contribute 1% to 2% of the L(TIR). The Herschel Dwarf Galaxy survey will provide statistical information on the nature of the dust and gas in low metallicity galaxies, elucidating the origin of the submm excess in dwarf galaxies, and help determine a ([CII] +CO) to H2 conversion factor, thus providing observational constraints on chemical evolution models of galaxies., Proceedings of the 5th Zermatt Symposium: "Conditions and Impact of Star Formation: New Results from Herschel and Beyond" September 19-24, 2010 Minor Language Corrections

Published
2011
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5. Infrared spectroscopy of NGC4151: Probing the obscured ionizing AGN continuum

Author

Alexander, Tal, Sturm, Eckhard, Lutz, Dieter, Sternberg, Amiel, Netzer, Hagai, and Genzel, Reinhard

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The ISO-SWS infrared spectroscopic observations of the nucleus of Seyfert galaxy NGC4151, which are described in a companion paper, are used together with a compilation of UV to IR narrow emission line data to determine the spectral shape of the obscured extreme-UV continuum that photoionizes the narrow line emitting gas in the active galactic nucleus. We present a new method to determine the best fitting photoionizing continuum and emission line cloud model from a heterogeneous set of emission line data. For NGC4151, we find a best-fit model that reproduces the observed line fluxes to within a factor of 2 on average, and which is consistent with the observed geometry of the optical Narrow Line Region (NLR). Our model consists of a clumpy, optically thick (ionization bounded) gas distribution, with a hydrogen gas density of ~1000 cm^-3 and a volume filling factor of 6.5*10^-4. Our best fitting spectral energy distribution (SED) falls sharply beyond the Lyman limit and then rises sharply again towards 100 eV. In particular, it does not display a `Big Blue Bump' signature of a hot accretion disk. We find that this SED, which best reproduces the NLR line emission on the 100--500 pc scale, does not have enough UV photons to produce the observed BLR recombination emission from the inner 1 pc. This suggests that the BLR is photoionized by the intrinsic continuum source, which does have a strong UV component (perhaps a Big Blue Bump), but that this UV component is absorbed by material located between the NLR and BLR. Our analysis suggests that the absorber consists of \~5*10^19 cm^-2 of neutral hydrogen. Such an absorber was independently detected by UV absorption lines (Kriss et al. 1992, 1995)., Comment: aastex, 55 pages, 18 figures. Accepted by ApJ

Published
1998
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6. From Clouds to Young Stellar Objects and back again: the all-in-one view from the Herschel infrared Galactic Plane Survey

Author

Molinari, Sergio, Abergel, Alain, Rivera-Ingraham, Alana, Noriega-Crespo, Alberto, Traficante, Alessio, Di Giorgio, Anna, Zavagno, Annie, Chrysostomou, Antonio, Roy, Arabino, Babar, Ali, Maiolo, Berlinda, Schulz, Bernhard, Jiang, Biwei, Sibthorpe, Bruce, Swinyard, Bruce, Battersby, Cara, Burigana, Carlo, Brunt, Chris, Davis, Chris, Joblin, Christine, Waelkens, Christoffel, Meny, Claude, Codella, Claudio, Popescu, Cristina, Polychroni, Danae, Eden, David, Ikhenaode, David, Elia, Davide, Paradis, Deborah, Shepherd, Debra, Russeil, Delphine, Ward-Thompson, Derek, Stamatellos, Dimitris, Marshall, Douglas, Sturm, Eckhard, Rosolowsky, Erik, Schisano, Eugenio, Faustini, Fabiana, Agostini, Fabio, Massi, Fabrizio, La Morgia, Federico, Piacentini, Francesco, Strafella, Francesco, Boulanger, Francois, Schuller, Frederic, Motte, Frederique, Wyrowski, Friedrich, Fuller, Gary, Gasperis, Giancarlo, Joncas, Gilles, Giardino, Giovanna, White, Glenn, Umana, Grazia, Lagache, Guilaine, Rivest, Guillaume, Stringfellow, Guy, Yorke, Harold, Ristorcelli, Isabelle, Difrancesco, James, Brand, Jan, Glenn, Jason, Kirk, Jason, Rodon, Javier, Baluteau, Jean-Paul, Bernard, Jean-Philippe, Li, Jinzeng, Neves, Joao, Mottram, Joe, Fischera, Joerg, Bally, John, Richer, John, Blommaert, Joris, Cernicharo, Jose, Ganga, Ken, Morgan, Larry, Testi, Leonardo, Anderson, Loren, Piazzo, Lorenzo, Campeggio, Loretta, Conversi, Luca, Olmi, Luca, Valenziano, Luca, Montier, Ludovic, Spinoglio, Luigi, Beltran, Maite, Huang, Maohai, Miville-Deschenes, Marc-Antoine, Sauvage, Marc, Veneziani, Marcella, Thompson, Mark, Cohen, Martin, Giard, Martin, Massimo Marengo, Compiegne, Mathieu, Griffin, Matt, Pomares, Melanie, Hoare, Melvin, Barlow, Michael, Burton, Michael, Reid, Michael, Smith, Michael, Pestalozzi, Michele, Juvela, Mika, Matsuura, Mikako, Benedettini, Milena, Schneider, Nicola, Billot, Nicolas, Peretto, Nicolas, Berne, Olivier, Caselli, Paola, Debernardis, Paolo, Natoli, Paolo, Saraceno, Paolo, Goldsmith, Paul, Garcia Lario, Pedro, Martin, Peter, Schilke, Peter, Lucas, Phil, Andre, Philippe, Royer, Pierre, Zhang, Qizhou, Plume, Rene, Cesaroni, Riccardo, Tuffs, Richard, Paladini, Roberta, Vavrek, Roland, Taylor, Russ, Carey, Sean, Viti, Serena, Masi, Silvia, Pezzuto, Stefano, Lord, Steve, Chakrabarti, Sukanya, Bontemps, Sylvain, Lim, Tanya, Mueller, Thomas, Robitaille, Thomas, Troost, Tobias, Moore, Toby, Minier, Vincent, Reach, William, and Fukui, Yasuo

Subjects
Settore FIS/05 - Astronomia e Astrofisica

8. The Spitzer/MIPS Star Formation Reference Survey

Author

Fazio, Giovanni, Ashby, Matthew, Ashby, Matthew L. N., Pauline Barmby, Chakrabarti, Sukanya, Gonzalez-Alfonso, Eduardo, Huang, Jia-Sheng, Madden, Suzanne, Noeske, Kai, Pahre, Michael, Papovich, Casey, Robitaille, Thomas, Smith, Howard, Sturm, Eckhard, Surace, Jason, Wang, Zhong, Whitney, Barbara, Willner, Steven, Wu, Hong, and Zezas, Andreas

9. First results from the JWST Early Release Science Program Q3D: Turbulent times in the life of a $z \sim 3$ extremely red quasar revealed by NIRSpec IFU

Author

Wylezalek, D, Vayner, A, Rupke, DSN, Zakamska, NL, Veilleux, S, Ishikawa, Y, Bertemes, C, Liu, W, Barrera-Ballesteros, JK, Chen, HW, Goulding, AD, Greene, JE, Hainline, KN, Hamann, F, Heckman, T, Johnson, SD, Lutz, D, Lützgendorf, N, Mainieri, V, Maiolino, R, Nesvadba, NPH, Ogle, P, Sturm, E, Wylezalek, D [0000-0003-2212-6045], Vayner, A [0000-0002-0710-3729], Rupke, DSN [0000-0002-1608-7564], Zakamska, NL [0000-0001-6100-6869], Veilleux, S [0000-0002-3158-6820], Ishikawa, Y [0000-0001-7572-5231], Bertemes, C [0000-0002-6948-1485], Liu, W [0000-0003-3762-7344], Barrera-Ballesteros, JK [0000-0003-2405-7258], Chen, HW [0000-0001-8813-4182], Goulding, AD [0000-0003-4700-663X], Greene, JE [0000-0002-5612-3427], Hainline, KN [0000-0003-4565-8239], Heckman, T [0000-0001-6670-6370], Johnson, SD [0000-0001-9487-8583], Lutz, D [0000-0003-0291-9582], Lützgendorf, N [0000-0002-4034-0080], Mainieri, V [0000-0002-1047-9583], Maiolino, R [0000-0002-4985-3819], Nesvadba, NPH [0000-0001-5783-6544], Ogle, P [0000-0002-3471-981X], Sturm, E [0000-0002-0018-3666], Apollo - University of Cambridge Repository, Wylezalek, Dominika [0000-0003-2212-6045], Vayner, Andrey [0000-0002-0710-3729], Rupke, David SN [0000-0002-1608-7564], Zakamska, Nadia L [0000-0001-6100-6869], Veilleux, Sylvain [0000-0002-3158-6820], Ishikawa, Yuzo [0000-0001-7572-5231], Bertemes, Caroline [0000-0002-6948-1485], Liu, Weizhe [0000-0003-3762-7344], Barrera-Ballesteros, Jorge K [0000-0003-2405-7258], Chen, Hsiao-Wen [0000-0001-8813-4182], Goulding, Andy D [0000-0003-4700-663X], Greene, Jenny E [0000-0002-5612-3427], Hainline, Kevin N [0000-0003-4565-8239], Heckman, Timothy [0000-0001-6670-6370], Johnson, Sean D [0000-0001-9487-8583], Lutz, Dieter [0000-0003-0291-9582], Lützgendorf, Nora [0000-0002-4034-0080], Mainieri, Vincenzo [0000-0002-1047-9583], Maiolino, Roberto [0000-0002-4985-3819], Nesvadba, Nicole PH [0000-0001-5783-6544], Ogle, Patrick [0000-0002-3471-981X], and Sturm, Eckhard [0000-0002-0018-3666]

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 5101 Astronomical Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, 51 Physical Sciences, Galaxies and Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Extremely red quasars, with bolometric luminosities exceeding $10^{47}$ erg s$^{-1}$, are a fascinating high-redshift population that is absent in the local universe. They are the best candidates for supermassive black holes accreting at rates at or above the Eddington limit, and they are associated with the most rapid and powerful outflows of ionized gas known to date. They are also hosted by massive galaxies. Here we present the first integral field unit (IFU) observations of a high-redshift quasar obtained by the Near Infrared Spectrograph (NIRSpec) on board the James Webb Space Telescope (JWST), which targeted SDSSJ165202.64+172852.3, an extremely red quasar at $z=2.94$. JWST observations reveal extended ionized gas - as traced by [OIII]$\lambda$5007\AA - in the host galaxy of the quasar, its outflow, and the circumgalactic medium. The complex morphology and kinematics imply that the quasar resides in a very dense environment with several interacting companion galaxies within projected distances of 10-15 kpc. The high density of the environment and the large velocities of the companion galaxies suggest that this system may represent the core of a forming cluster of galaxies. The system is a good candidate for a merger of two or more dark matter halos, each with a mass of a few $10^{13}$ M$_\odot$ and traces potentially one of the densest knots at $z\sim3$., Comment: ApJL in press, 11 pages, please also see associated ESA / STScI press release from Oct 20th 2022

Published
2022
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